MN is supported by a Royal Astronomical Society Research Fellowship. Gomez is partly supported by an NSF Graduate Research Fellowship. The Berger Time-Domain Group at Harvard is supported in part by NSF under grant AST-1714498 and by NASA under grant NNX15AE50G. Mockler for useful discussions regarding the MOSFiT TDE model and an anonymous referee for comments towards the improvement of this paper. The photometry shown here is available on the online version of this journal. The black lines mark the times for which we have optical spectra (Short et al. Optical and UV light curves of AT 2018hyz, host-subtracted and corrected for galactic extinction. under cooperative agreement with the National Science Foundation. The low optical depth implied by the small debris mass may explain how we are able to see hydrogen emission with disc-like line profiles in the spectra of AT2018hyz (see our companion paper).ĢIRAF is written and supported by the National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc. We model the optical and UV light curves using the Modular Open-Source Fitter for Transients (MOSFiT) and find a best fit for a black hole of 5.2 × 106 M0 disrupting a 0.1 M0 star the model suggests the star was likely only partially disrupted, based on the derived impact parameter of ß = 0.6. A thermal X-ray model is unable to account for photons > 1 keV, while a radio non-detection favours inverse-Compton scattering rather than a jet for the non-thermal component. The X-ray spectrum shows a total unabsorbed flux of ~4 × 10-14 erg cm -2 s-1 and is best fit by a blackbody plus power-law model with a photon index of r = 0.8. We detect a constant X-ray source present for at least 86 d. An excess bump appears in the UV light curve about 50 d after bolometric peak, followed by a flattening beyond 250 d. The bolometric light curve of AT 2018hyz is comparable to other known TDEs and declines at a rate consistent with a t-5/3 at early times, emitting a total radiated energy of E = 9 × 1050 erg. We present optical+UV photometry of the transient, as well as an X-ray spectrum and radio upper limits. The pipeline is controlled through the user friendly SAOImage DS9 package.AT 2018hyz (= ASASSN-18zj) is a tidal disruption event (TDE) located in the nucleus of a quiescent E+A galaxy at a redshift of z = 0.04573, first detected by the All-Sky Automated Survey for Supernovae (ASAS-SN). Our pipeline uses a modular design so that it can be easily implemented or customized as a real-time robotic telescope pipeline on any observatory. Other observers can then monitor the data stream in real time and make an informed decision whether to perform complementary observations of a transient event in progress. An observer using this resource can automatically stream photometric data over the Internet. ![]() The pipeline is controlled through the user friendly SAOImage DS9 package.ĪB - We present a new automated photometric pipeline optimized for time-series photometry that includes a real-time data streaming service. ![]() ![]() N2 - We present a new automated photometric pipeline optimized for time-series photometry that includes a real-time data streaming service. T1 - Implementing a real-time data stream for time-series stellar photometry
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